2 ABSTRACT We assess the contribution of solar forcing from the interplanetary magnetic field (IMF) B and solar wind velocity (Vsw) on the auroral inputs from intercalibrated NOAA and DMSP satellite-track in-situ particle measurements. Periodicities in Vsw and the global electron (Pe) and ion power (Pi) are calculated using Lomb-Scargle (L-S) and wavelet analyses. We examine two different solar minimum periods in a broader context, including radiation belt electrons >2 MeV. The first Whole Sun Month (WSM) interval ( ) had a strong solar magnetic dipole. Strong 'semiannual' equinoctial periodicities of ~20% variation in Vsw and 40% variation in Pe were found. In the present solar minimum, the solar magnetic field is weaker with larger quadrupole components during the Whole Heliospheric Interval (WHI, ). Strong 9-d amplitudes of ~30% variation in Vsw and ~40% variation in Pe and Pi were found. This 9-d periodicity was also found in the IMF B, in the CHAMP neutral density at 400 km, and in the outer radiation belt electrons >2 MeV. Solar periodicities are also examined using the available parameters during previous solar minima in and in

3 Estimates of the electron hemispheric power (HPe) into the auroral regions from particle detectors on NOAA and DMSP satellites were inter-calibrated over 31 years and 24 satellites.

4 The electron hemispheric power (HPe) is found in both hemispheres on an hourly basis. The sum of the Northern and Southern hemispheres is the auroral electron power (Pe). Uncalibrated HPe Calibrated HPe

5 The ion hemispheric power (HPi) is found from 5 NOAA SEM-2 satellites as HPi=Hpt-Hpe (<20keV) Arrows show high voltage gain increases for N16. Baseline is set to N12 or ~2x too high. old new real values; baseline increased to agree with DMSP ions <20 kev

10 Correlation of Pe with Vsw B Transient fit higher than HSS+slow for Bz<0, lower for Bz>0, so an increase in B (or Bz) is more,less effective for Bz<0,>0.

11 Solar Rotational Periodicities in the total Vsw, Pe, and Pi Largest amplitudes in Descending (D) and Minimum (N) phases of the solar cycle.

12 Two Solar Minimum Comparisons

13 1996 WSM and 2008 WHI Minima SOHO/EIT images (a-d) show coronal holes as dark regions in extreme-ultraviolet emission. Radiation belt electrons >2 MeV (i-j) initially decrease with pressure pulses at the leading edges of HSS, and then are high until the next leading edge pressure pulse. [Gibson et al., JGR, 2009]

14 WSM and WHI in Context Vsw in dark blue shows an increase of ~8% from WSM to WHI. The sunspot cycle is similar to the solar wind B field in (a), and decreases ~15% between WSM and WHI. The solar wind density (Dsw) in (b) shows a stronger decrease of ~35%. Pe in (c) is nearly coincident with Vsw except it decreases ~5% from WSM to WHI because of the decrease in B. The radiation belt electrons in (d) increases, possibly because of lower loss rates (Dsw less).

15 Magnetic field (-15%) & Solar wind speed (+8%) -15% Vsw in dark blue shows an increase of ~8% from WSM to WHI. The sunspot cycle is similar to the solar wind B field in (a), and decreases ~15% between WSM and WHI. The solar wind density (Dsw) in (b) shows a stronger decrease of ~35%. Pe in (c) is nearly coincident with Vsw except it decreases ~5% from WSM to WHI because of the decrease in B. The radiation belt electrons in (d) increases, possibly because of lower loss rates (Dsw less).

16 Solar wind density (-35%) & Solar wind speed (+8%) -35% Vsw in dark blue shows an increase of ~8% from WSM to WHI. The sunspot cycle is similar to the solar wind B field in (a), and decreases ~15% between WSM and WHI. The solar wind density (Dsw) in (b) shows a stronger decrease of ~35%. Pe in (c) is nearly coincident with Vsw except it decreases ~5% from WSM to WHI because of the decrease in B. The radiation belt electrons in (d) increases, possibly because of lower loss rates (Dsw less).

17 Auroral Power (-5%) & Solar wind speed (+8%) -5% Vsw in dark blue shows an increase of ~8% from WSM to WHI. The sunspot cycle is similar to the solar wind B field in (a), and decreases ~15% between WSM and WHI. The solar wind density (Dsw) in (b) shows a stronger decrease of ~35%. Pe in (c) is nearly coincident with Vsw except it decreases ~5% from WSM to WHI because of the decrease in B. The radiation belt electrons in (d) increases, possibly because of lower loss rates (Dsw less).

18 Radiation belt (x3.4) & Solar wind speed (+8%) X3.4 Vsw in dark blue shows an increase of ~8% from WSM to WHI. The sunspot cycle is similar to the solar wind B field in (a), and decreases ~15% between WSM and WHI. The solar wind density (Dsw) in (b) shows a stronger decrease of ~35%. Pe in (c) is nearly coincident with Vsw except it decreases ~5% from WSM to WHI because of the decrease in B. The radiation belt electrons in (d) increases, possibly because of lower loss rates (Dsw less).

27 Solar Forcing Transients contribute ~40% and ~6% to Pe in solar maximum and minimum, respectively. Transients represent the largest B values, and are more effective in producing Pe during Bz negative conditions, and less effective in producing Pe during Bz positive conditions than HSS and slow-speed wind. HSS contribute ~57% and ~32% to Pe in descending and solar maximum phases. HSS determine the structure of the total Vsw or Pe, and contribute the most to periodicities. Solar minima in 1996 and 2008 are different in solar magnetic fields, coronal hole distributions, Vsw distributions and periodicities, and solar wind densities which lead to profound effects in the Earth s radiation belts, aurora, magnetic activity, and upper atmosphere. The semi-annual amplitudes from Lomb analyses were large ~ for Vsw and Pe. In ~1996 (WSM), the Vsw sa periods peaked in the equinoxes, enhancing the normal equinoctial peaks in Pe from Russell- McPherron mechanisms, etc. The semi-annual amplitudes were absent or weak ~ (WHI). The 9-day periodicities in Vsw (especially in HSS), Pe and Pi seen after 2003 were strong in 2005 and 2008 (WHI), and were absent or weak ~ (WSM). They are also present in Kp, the neutral thermosphere density in WHI, TEC (Lei et al., GRL, 2008), and infrared [NO] and [CO2] cooling (Mlynczak et al., GRL, 2008), and are absent or weak in SEE flux, and 10.7 cm solar flux (Lei et al., JGR, 2008). 9-day periods also in 1976 and 1983.

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